Beyond the general behavior of \(\tilde{\Lambda }\)  that we studied above, it is in our interest to examine the radius and possible constraints that can be derived from it. Following the previous steps, we focus on the \(R_{1.4}\)  case of a \(m_2=1.4\;M_\odot \)  secondary component neutron star. In Fig. REF  we display this dependence; the EoSs are in five main groups, characterized by the transition density \(n_{\mathrm {tr}}\) . We notice that we expanded our study to transition densities \(n_{\mathrm {tr}}=[1.25,1.75,2.25]\)  to be more accurate in calculations and study in more detail the curves' behavior. The higher speed of sound values correspond to lighter marks' color. In analog to the remarks of the previous Fig. REF , the high speed of sound bounds lead to higher \(\tilde{\Lambda }\)  and \(R_{1.4}\) . Moreover, we applied a fitting expression to the \((v_s/c)^2=[0.8,0.9,1]\)  cases. The expression was taken to be in the kind of the proposed relations of Refs. [1]}, [2]}.
\(\tilde{\Lambda }=c_5R^{c_6}_{1.4},\) 
